Here we show the output files from the models used in Cerviño et al. (2000) paper about 26Al and 60Fe.:
The data files contains:
- Age in Myrs
- log NHlyc: log of the number of Q(H0) photons s-1 Mo-1
- log NHelyc: log of the number of Q(He0) photons s-1 Mo-1
- # O, # WR, # WN, # WC, # RSG, # SN: Number of different types of stars in Mo-1
- M_0: Initial mass of the most massive star in the cluster.
- M_t: Current mass of the most massive star in the cluster.
- 26Al*tot, 26Al*, 26Alwr, 26AlSnI, 26AlSNII, 26AlSN, 26Al: Masses of 26Al emitted by all stars, non-WR stars, WR, SN I, SN II, all SN, and stars+SN in units of MoAl Myr-1 Mo-1. It corresponds to ydot26 in the paper.
- 60FeSnI, 60FeSNII, 60Fe: Masses of 60Fe emitted by SN I, SN II, and all SN in units of MoFe Myr-1 Mo-1. It corresponds to ydot60 in the paper.
- 26Aldec, Fe60dec: Emissivities (decay reates, Ydot in the paper, related with the flux of the line) of 26Al and 60Fe in Mo Myr-1 Mo-1.
For use it you must multiply the output by the ammount of gas transformed in stars, and you must take into account that:
- The models assume a Salpeter IMF slope in the mass range 2 - 120 Mo, so the multiply factor is the ammount of gas transformed in stars in this mass range.
- The output has been normalized to:
- Instantaneous Burst (IB) case:
The amount of gas transformed in stars
since the onset of the burst
(click here to get the IB table) - CSFR:
The amount of gas transformed in stars
since the onset of the burst:
- If you have a CSFR of 1Mo/yr and the burst have an age of 20Myrs, you must multiply by 1Mo/yr x 20 106Myrs = 2 107Mo.
- If you do not know the age, multiply each observable by the age (collumn 1). The resulting table is then normalized by a CSFR = 1Mo/Myr. The final ages must show a constant value with time and you can use it (assuming that it is an equilibrium value).
- Instantaneous Burst (IB) case:
The amount of gas transformed in stars
since the onset of the burst
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Miguel Cerviño 2001